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dc.rights.license© ESO 2020-
dc.contributor.authorYang, C.-
dc.contributor.authorGonzález Alfonso, E.-
dc.contributor.authorOmont, A.-
dc.contributor.authorPereira Santaella, M.-
dc.contributor.authorFischer, J.-
dc.contributor.authorBeelen, A.-
dc.contributor.authorGavazzi, R.-
dc.contributor.otherUnidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737-
dc.identifier.citationAstronomy and Astrophysics 634: L3(2020)es
dc.description.abstractSubmillimeter rotational lines of H2O are a powerful probe in warm gas regions of the interstellar medium (ISM), tracing scales and structures ranging from kiloparsec disks to the most compact and dust-obscured regions of galactic nuclei. The ortho-H2O(423 − 330 line at 448 GHz, which has recently been detected in a local luminous infrared galaxy, offers a unique constraint on the excitation conditions and ISM properties in deeply buried galaxy nuclei because the line requires high far-infrared optical depths to be excited. In this letter, we report the first high-redshift detection of the 448 GHz H2O(423–330) line using ALMA in a strongly lensed submillimeter galaxy (SMG) at z = 3.63. After correcting for magnification, the luminosity of the 448 GHz H2O line is ∼106 L⊙. In combination with three other previously detected H2O lines, we build a model that resolves the dusty ISM structure of the SMG, and find that it is composed of a ∼1 kpc optically thin (optical depth at 100 μm τ100 ∼ 0.3) disk component with a dust temperature Tdust ≈ 50 K that emits a total infrared power of 5 × 1012 L⊙ with a surface density ΣIR = 4 × 1011 L⊙ kpc−2, and a very compact (0.1 kpc) heavily dust-obscured (τ100 ≳ 1) nuclear core with very warm dust (100 K) and ΣIR = 8 × 1012 L⊙ kpc−2. The H2O abundance in the core component, XH2O ∼ (0.3–5) × 10−5, is at least one order of magnitude higher than in the disk component. The optically thick core has the characteristic properties of an Eddington-limited starburst, providing evidence that radiation pressure on dust is capable of supporting the ISM in buried nuclei at high redshifts. The multicomponent ISM structure revealed by our models illustrates that dust and molecules such as H2O are present in regions that are characterized by highly differing conditions and scales, extending from the nucleus to more extended regions of
dc.description.sponsorshipWe thank the anonymous referee for very helpful suggestions. C.Y. acknowledges support from an ESO Fellowship. E.G.-A. is a Research Associate at the Harvard-Smithsonian Center for Astrophysics, and thanks the Spanish Ministerio de Economia y Competitividad for support under project ESP2017-86582-C4-1-R. E.G.-A. also thanks the support from the ESO Chile Scientific Visitor Programme. M.P.S. acknowledges support from the Comunidad de Madrid through Atraccion de Talento Investigador Grant 2018-T1/TIC-11035. This paper makes use of the following ALMA data: ADS/JAO.ALMA 2018.1.00797.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. ; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737).es
dc.publisherEDP Scienceses
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/ESP2017-86582-C4-1-R/ES/CONTRIBUCION ESPAÑOLA A LAS MISIONES ESPACIALES CRIOGENICAS SPICA Y ATHENA, POST-OPERACIONES DE HERSCHEL Y EXPLOTACION CIENTIFICA MULTIFRECUENCIA/-
dc.rightsAttribution-NonCommercial-NoDerivatives 4.0 International*
dc.subjectGalaxies: high redshiftes
dc.subjectGalaxies: ISMes
dc.subjectInfrared: galaxieses
dc.subjectSubmillimeter: galaxieses
dc.subjectRadio lines: ISMes
dc.subjectISM: moleculeses
dc.titleFirst detection of the 448 GHz ortho-H2O line at high redshift: probing the structure of a starburst nucleus at z =
dc.contributor.orcidGavazzi, R. [0000-0002-5540-6935]-
dc.contributor.orcidYang, C. [0000-0002-8117-9991]-
dc.contributor.orcidFischer, J. [0000-0001-6697-7808]-
dc.contributor.funderAgencia Estatal de Investigación (AEI)-
dc.contributor.funderComunidad de Madrid-
dc.description.peerreviewedPeer reviewes
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